Volume 442, Number 1, October IV 2005
|Page(s)||29 - 41|
|Section||Cosmology (including clusters of galaxies)|
|Published online||30 September 2005|
Internal dynamics of the z ~ 0.8 cluster RX J0152.7-1357
Dipartimento di Astronomia, Università degli Studi di Trieste, via Tiepolo 11, 34100 Trieste, Italy e-mail: email@example.com
2 ESO-European Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany
3 Department of Physics & Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA
Accepted: 1 June 2005
We present the results from the dynamical analysis of the cluster of galaxies RX J0152.7-1357, which shows a complex structure in its X-ray emission, with two major clumps in the central region and a third clump in the Eastern region. Our analysis is based on redshift data for 187 galaxies. We find that RX J0152.7-1357 appears as a well isolated peak in the redshift space at , which includes 95 galaxies recognized as cluster members. We compute the line-of-sight velocity dispersion of galaxies, km s-1, which is significantly larger than what is expected in the case of a relaxed cluster with an observed X-ray temperature of 5-6 keV. We find evidence that this cluster is far from dynamical equilibrium, as shown by the non Gaussianity of the velocity distribution, the presence of a velocity gradient and a significant substructure. Our analysis shows that the high value of is due to the complex structure of RX J0152.7-1357, i.e. to the presence of three galaxy clumps of different mean velocities. Using optical data we detect a low-velocity clump (with –500 km s-1) in the central southwest region and a high-velocity clump (with km s-1) in the Eastern region, corresponding well to the South–West and East peaks detected in the X-ray emission. The central North–East X-ray peak is associated to the main galaxy structure with a velocity which is intermediate between those of the other two clumps and km s-1. The mass of the whole system within 2 Mpc is estimated to lie in the range , depending on the model adopted to describe the cluster dynamics. Such values are comparable to those of very massive clusters at lower redshifts. Analytic calculations based on the two-body model indicate that the system is most likely bound and currently undergoing merging. In particular, we suggest that the southwestern clump is not a small group, but rather the dense cluster-core of a massive cluster, most likely destined to survive tidal disruption during the merger.
Key words: galaxies: clusters: general / galaxies: clusters: individual: RX J0152.7-1357 / galaxies: distances and redshifts / cosmology: observations
© ESO, 2005
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